THE coronal emission lines are produced by highly ionized atoms undergoing forbidden transitions from metastable levels1. In an attempt to identify further lines we have examined the level separation 3P2—3P1 in the excited four-electron configuration 1s2 2s 2p. Fig. 1 shows the level structure near the ground-state.
For a review see Edlén, B., Mon. Not. Roy. Astro. Soc., 105, 323 (1945). More recent identifications are given in Intern. Astro. Union Symp., 16, Cloudcroft, 1961, The Solar Corona, edit. by Evans, J. W., 286 (1963).
Layzer, D., Ann. Phys. (New York), 8, 271 (1959); 17, 177 (1962).
Moore, C. E., Atomic Energy Levels, Nat. Bur. Stand. Circ., 467 (1949). Bockasten, K., Hallin, R., and Hughes, T. P., Proc. Phys. Soc., 81, 522 (1963).
Aly, M. K., Astrophys. J., 122, 438 (1955). Aly, M. K., in the Cloudcroft Symp. (ref. 1), 285.
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COLLINS, P., PRYCE, M. Identification of Solar Coronal Emission Lines. Nature 202, 1319 (1964). https://doi.org/10.1038/2021319a0
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